Protoneutron Star Cooling with Convection: The Effect of the Symmetry Energy
Abstract
We model neutrino emission from a newly born neutron star subsequent to a supernova explosion to study its sensitivity to the equation of state, neutrino opacities, and convective instabilities at high baryon density. We find the time period and spatial extent over which convection operates is sensitive to the behavior of the nuclear symmetry energy at and above nuclear density. When convection ends within the protoneutron star, there is a break in the predicted neutrino emission that may be clearly observable.
- Publication:
-
Physical Review Letters
- Pub Date:
- February 2012
- DOI:
- 10.1103/PhysRevLett.108.061103
- arXiv:
- arXiv:1112.0335
- Bibcode:
- 2012PhRvL.108f1103R
- Keywords:
-
- 26.50.+x;
- 21.65.Mn;
- 26.60.-c;
- 97.60.Bw;
- Nuclear physics aspects of novae supernovae and other explosive environments;
- Equations of state of nuclear matter;
- Nuclear matter aspects of neutron stars;
- Supernovae;
- Astrophysics - High Energy Astrophysical Phenomena
- E-Print:
- 4 Pages, 3 Figures, Accepted to PRL